1. Why include binary interactions in EPS models?

Why include binary interactions in EPS models? Binary interactions can create some classes of luminous and blue objects, such as subdwarf B stars (sdBs) and blue stragglers (BSs). These stars can raise the flux in the UV band. The UV flux is an important SFR tracer. Moreover, the UV flux can been seen in the visible band when redshift z is ~2.

2. Which kinds of objects are created by binary interactions in Yunnan models?

Binary interactions can create sdBs, BSs, symbiotic stars, and so on. Moreover, Han et al. (2002, 2003) have proposed a binary model for the formation of hot sdBs in binaries and single hot sdBs, and Han et al. (2007) presented the ISEDs of populations with the binary interactions of sdB. Therefore, we presented the new set of ISEDs for SPs comprising sdBs.

3. Results

a) SPs (stellar populations)

The stellar mass, magnitudes, mass-to-light ratios, ISEDs and Lick/IDS indices are provided for SP with and without binary interactions. Age: from 1.e+6 to 1.5e+10 yr. Metallicity: from 1.e-4 [or 4.e-3] to 0.03.

------ ISED: at three resolutions (8-20Å [based on BaSeL stellar spectra library], 0.3Å [HRES] and 0.1Å [BLUERED]).

------ stellar mass & magnitudes: 48 magnitudes, including bolometric magnitude, GALEX (Fuv, Nuv), SDSS (u, g, r, i, z), Johnson (U, B, V, R, I), 2MASS (J, H, K) and HST-WFPC2 (f122m-f1042m, 32 filters) magnitudes.

------ mass-to-light ratios: 8 mass-to-light ratios.

------ Lick/IDS indices: 25 indices, including from CN1 to HγF. The results are obtained by both empirical fitting function (FF) and direct computation (DC) methods.

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b) SPs (comprising the BIs of sdBs by Han et al. 2007)

Based on the ISEDs for SPs with binary interactions, we combine the ISEDs of SPs with the binary interactions of sdB (Han et al. 2007) and present the stellar mass, magnitudes, mass-to-light ratios, low-resolution ISEDs for SPs with BIs. Age: from 1.e+6 to 1.5e+10 yr. Metallicity: from 1.e-4 to 0.03.

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c) CSPs (composite stellar populations)

We also provide the ISEDs of composite SPs (13 types), including E, S0, Sa-Sd, Irr types of galaxy and five other types (with short e-folding timescale). Age: from 1.e+6 to 1.5e+10 yr. Metallicity: from 1.e-4 to 0.03.

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d) CSP + nebula systems

Moreover, we provide the stellar, nebular, total spectra, the luminosities of spectral lines (Hα, Hβ) and the number of ionizing photons for the CSP+nebula systems (13 types), including E, S0, Sa-Sd, Irr galaxy types and five other galaxy types (with short e-fold timescale). Age: from 1.e+6 to 1.5e+10 yr. Metallicity: from 1.e-4 to 0.03.

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e) Sole effect of binary interactions on SPs, CSPs and CSP+nebula systems

In order to include the effect of binary interactions in other EPS models, we also present the sole effect of binary interactions on the results of SPs, CSPs and CSP+nebula systems.

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4. Code and Format

The ISEDs have the same format as that of BC03 models. We also provide the code used to read these data.